Optical observations of SS 433 during eclipses - Structure of the accretion disk

Details Optical observations of SS 433 during eclipses - Structure of the accretion disk Optical observations of SS 433 during eclipses - Structure of the accretion disk

Oct 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997azh....74..740g&link_type=abstract

Astronomicheskij Zhurnal, vol. 74, p. 740

Astronomy and Astrophysics

Astronomy

Variable Stars, X Ray Sources, Radio Stars, Accretion Disks, Eclipsing Binary Stars, Stellar Structure, Ubv Spectra, Stellar Spectrophotometry, Helium, Visual Observation

Scientific paper

The results of photometric UBVRI, H-alpha, and spectral observations of SS 433 during eclipses of the accretion disk are presented. The He II emission originates near the accretion disk, and has two components - a narrow, nearly Gaussian profile with width FWHM of about 1000 km/s and a broad two-peaked profile. The regions where the narrow He II component and the H-beta line are emitted experience partial eclipses at orbital phases 0.1 and 0.1-0.2, respectively, which indicates that these lines originate in a gaseous flow to the accretion disk. The broad He II line is completely eclipsed at phase 0.0. The blue and red wing components of this line are probably formed in gaseous cocoons around the bases of the relativistic jets. The gas flow velocity in the cocoons is equal to about 1500 km/s. The size of the He II cocoon is 0.25-0.30 times the radius of the orbit; an X-ray emitting region with size 0.20 lies inside this cocoon. The He II region outside the outwardly propagating jets is not shadowed by the accretion disk, but experiences total eclipses by the optical star of the system.

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